Quasilocal energy for rotating charged black hole solutions in general relativity and string theory

Details Quasilocal energy for rotating charged black hole solutions in general relativity and string theory Quasilocal energy for rotating charged black hole solutions in general relativity and string theory

1999-11-10

arxiv.org/abs/hep-th/9911070v1

Phys.Rev.D60:104027,1999

Physics

High Energy Physics

High Energy Physics - Theory

15 pages

Scientific paper

10.1103/PhysRevD.60.104027

We explore the (non)-universality of Martinez's conjecture, originally proposed for Kerr black holes, within and beyond general relativity. The conjecture states that the Brown-York quasilocal energy at the outer horizon of such a black hole reduces to twice its irreducible mass, or equivalently, to \sqrt{A} /(2\sqrt{pi}), where `A' is its area. We first consider the charged Kerr black hole. For such a spacetime, we calculate the quasilocal energy within a two-surface of constant Boyer-Lindquist radius embedded in a constant stationary-time slice. Keeping with Martinez's conjecture, at the outer horizon this energy equals the irreducible mass. The energy is positive and monotonically decreases to the ADM mass as the boundary-surface radius diverges. Next we perform an analogous calculation for the quasilocal energy for the Kerr-Sen spacetime, which corresponds to four-dimensional rotating charged black hole solutions in heterotic string theory. The behavior of this energy as a function of the boundary-surface radius is similar to the charged Kerr case. However, we show that in this case it does not approach the expression conjectured by Martinez at the horizon.

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